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Hot Jupiters with Relatives: Discovery of Additional Planets in Orbit Around WASP-41 and WASP-47?,??

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Hot Jupiters with Relatives: Discovery of Additional Planets in Orbit Around WASP-41 and WASP-47?,?? A&A 586, A93 (2016) Astronomy DOI: 10.1051/0004-6361/201526965 & c ESO 2016 Astrophysics Hot Jupiters with relatives: discovery of additional planets in orbit around WASP-41 and WASP-47?;?? M. Neveu-VanMalle1;2, D. Queloz2;1, D. R. Anderson3, D. J. A. Brown4, A. Collier Cameron5, L. Delrez6, R. F. Díaz1, M. Gillon6, C. Hellier3, E. Jehin6, T. Lister7, F. Pepe1, P. Rojo8, D. Ségransan1, A. H. M. J. Triaud9;10;1, O. D. Turner3, and S. Udry1 1 Observatoire Astronomique de l’Université de Genève, Chemin des Maillettes 51, 1290 Sauverny, Switzerland e-mail: [email protected] 2 Cavendish Laboratory, J J Thomson Avenue, Cambridge, CB3 0HE, UK 3 Astrophysics Group, Keele University, Staffordshire, ST5 5BG, UK 4 Department of Physics, University of Warwick, Gibbet Hill Road, Coventry CV4 7AL, UK 5 SUPA, School of Physics and Astronomy, University of St. Andrews, North Haugh, Fife, KY16 9SS, UK 6 Institut d’Astrophysique et de Géophysique, Université de Liège, Allée du 6 Août, 17, Bat. B5C, 19C 4000 Liège 1, Belgium 7 Las Cumbres Observatory Global Telescope Network, 6740 Cortona Dr. Suite 102, Goleta, CA 93117, USA 8 Departamento de Astronomía, Universidad de Chile, Camino El Observatorio 1515, Las Condes, Santiago, Chile 9 Centre for Planetary Sciences, University of Toronto at Scarborough, 1265 Military Trail, Toronto, ON, M1C 1A4, Canada 10 Department of Astronomy & Astrophysics, University of Toronto, Toronto, ON, M5S 3H4, Canada Received 14 July 2015 / Accepted 30 September 2015 ABSTRACT We report the discovery of two additional planetary companions to WASP-41 and WASP-47. WASP-41 c is a planet of minimum mass 3.18 ± 0.20 MJup and eccentricity 0.29 ± 0.02, and it orbits in 421 ± 2 days. WASP-47 c is a planet of minimum mass 1.24 ± 0.22 MJup and eccentricity 0.13 ± 0.10, and it orbits in 572 ± 7 days. Unlike most of the planetary systems that include a hot Jupiter, these two systems with a hot Jupiter have a long-period planet located at only ∼1 au from their host star. WASP-41 is a rather young star known to be chromospherically active. To differentiate its magnetic cycle from the radial velocity effect induced by the second planet, we used the emission in the Hα line and find this indicator well suited to detecting the stellar activity pattern and the magnetic cycle. The analysis of the Rossiter-McLaughlin effect induced by WASP-41 b suggests that the planet could be misaligned, though an aligned orbit cannot be excluded. WASP-47 has recently been found to host two additional transiting super Earths. With such an unprecedented architecture, the WASP-47 system will be very important for understanding planetary migration. Key words. stars: individual: WASP-47 – stars: individual: WASP-41 – techniques: photometric – techniques: radial velocities – techniques: spectroscopic – planetary systems 1. Introduction between 0.8 and 5 au (Curiel et al. 2011). Ten years later, the dis- covery of the planetary system around HIP 14810 (Wright et al. In contrast to the large number of multiple planetary systems, 2007, 2009) revealed that a hot Jupiter can be found in a system stars with hot-Jupiter planets have long been thought to lack ad- with smaller planets on wider orbits. From 15 years of radial ve- ditional planets. Recent studies suggest that this statement may locity surveys, Feng et al.(2015) recently constrained the orbits not be true (e.g. Knutson et al. 2014). However the existence of of the distant (P > 9 years) giant planets in orbit around the hot- those additional planets was revealed by nothing more than ra- Jupiter hosts HD 187123 and HD 217107. Among all systems dial velocity trends. Only seven outer planetary companions of with a close-in giant planet discovered by transit surveys, only close-in (a < 0:1 au) giant planets have a full orbital period that HAT-P-13 (Bakos et al. 2009), HAT-P-46 (Hartman et al. 2014), has been observed. and Kepler-424 (Endl et al. 2014) have an additional planetary The multiple planetary system around υ Andromedae (Butler companion detected by Doppler surveys with a fully measured et al. 1997) was the first to be found with a hot Jupiter. This orbit. planet is surrounded by three more massive giant planets orbiting The Wide Angle Search for Planets (WASP, Pollacco et al. ? Using data collected at ESO’s La Silla Observatory, Chile: HARPS 2006) has discovered more than 100 hot Jupiters. While some on the ESO 3.6 m (Prog ID 087.C-0649 & 089.C-0151), the Swiss of them clearly have a very distant companion (e.g. WASP-8, Euler Telescope, TRAPPIST, the 1.54-m Danish telescope (Prog Queloz et al. 2010), none of them were previously known to have CN2013A-159), and at the LCOGT’s Faulkes Telescope South. a fully resolved orbit. ?? Photometric lightcurve and RV tables are only available at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) The radial velocity follow-up observations of WASP initi- or via ated in 2008 with the fibre-fed echelle spectrograph CORALIE http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/586/A93 (mounted on the 1.2-m Euler Swiss telescope at La Silla) has Article published by EDP Sciences A93, page 1 of 12 A&A 586, A93 . (2016) . identified new multiple systems including a hot Jupiter. We re- 0.6 port here the detection of additional planets around WASP-41 (Maxted et al. 2011) and WASP-47 (Hellier et al. 2012). These 0.5 new planets are both located only ∼1 au of their parent star. 0.4 When searching for long-period companions using the radial ve- 0.3 locities technique, the effects of stellar activity should be care- 0.2 Normalised power fully considered to avoid misdetections. A stellar magnetic cycle Normalized power 0.1 may mimic the signal of a planetary companion (e.g. Lovis et al. 0.0 2011). WASP-41 is known to be active (Maxted et al. 2011), 2.5.10.0 20. 50. 100.0 200. 500. 1000. which makes it important to recognise the temporal structure of . Period [days] . its magnetic cycle. Since the photospheric Ca (H & K) emission lines cannot be extracted from single CORALIE spectra (insuffi- Fig. 1. WASP-47 Lomb-Scargle periodogram of the residuals after sub- cient signal-to-noise ratio), we alternatively use the emission in tracting Planet b. The dotted lines correspond to a false-alarm probabil- the Hα band to characterise activity. We find that this indicator ity of 0.1%, 1%, and 10%. is very well suited to WASP-41, though it may not be true in general (Cincunegui et al. 2007). Monte-Carlo (MCMC) fitting scheme to derive the system pa- Section2 reports the observations, analysis, and results for rameters of the two-planet model. We did not include the WASP WASP-47. Section3 similarly addresses the case of WASP-41 photometry in our analysis because it has poor precision com- with a description of the various additional observations, a study pared to EulerCAM and might suffer from spatial dilution from of the stellar activity, and an analysis that includes the Rossiter- background stars. We used the most recent version of the code McLaughlin effect followed by the results. In Sect.4, after dis- described in Gillon et al.(2012) and references therein. The cussing the importance of considering magnetic cycles when jump parameters used in our analysis to characterise the tran- searching for long-period planets, we compare our two multi- siting planet WASP-47b were ple planetary systems, including a hot Jupiter, to the five previ- ously known ones. We discuss the biases induced by the observ- – the transit depth defined as the planet/star area ratio (dF = 2 ing strategies of Doppler and transit surveys in finding multiple (Rp=R?) ), where Rp and R? are the planetary and stellar ra- planetary systems including a hot Jupiter. Finally we check the dius, respectively; transit probabilities of WASP-47c and WASP-41c. – the transit impact parameter in the case of a circular orbit 0 During the process of revision of this paper, Becker et al. (b = ab cos ip;b=R?), where ab and ip;b are the semi-major (2015) reported the presence of two additional super-Earths tran- axis and the inclination of the planetary orbit, respectively; siting WASP-47 every ∼0.8 and 9 days. This remarkable discov- – the transit duration T14, from first to last contact; ery brings strong constraints on the migration of this system and – the orbital period Pb; will be discussed in the last section. – the time of inferior conjunctionp T0;b; p – the two parameters eb cos !b and eb sin !b, where eb is the eccentricity and !b the argument of periastron; 2. WASP-47 c q − 2 1=3 – the parameter K2;b = Kb 1 eb Pb , where Kb is the radial 2.1. Observations velocity semi-amplitude. WASP-47 is a G9V star hosting a giant planet with a mass of For the period Pb and time of inferior conjunction T0;b, we im- 1.14 MJup and a period of 4.16 days (Hellier et al. 2012). The posed Gaussian priors defined by the values derived in Hellier discovery paper includes 19 radial velocity measurements taken et al.(2012), since we did not include the WASP photometry in with CORALIE during two observing seasons. Ongoing moni- our analysis. Uniform priors were assumed for the probability toring revealed a possible third body, and after 46 observations distribution functions (PDFs) of all the other jump parameters.
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